introduction to km3net science · prof. dr. harold yepes ramírez, nnn2019, medellÍn-colombia...

Prof. Dr. Harold Yepes Ramírez

KM3NeT-EC PRINCIPAL INVESTIGATOR

LASF4RI NATIONAL REPRESENTATIVE

20TH INTERNATIONAL WORKSHOP ON NEXT GENERATION NUCLEON DECAY AND NEUTRINO DETECTORS

MEDELLÍN – COLOMBIA

7-9TH NOVEMBER 2019

INTRODUCTION TO KM3NeT SCIENCE

THE KM3NeT NEUTRINO DETECTOR

KM3NeT PERFORMANCE

KM3NeT FIRST DATA AND FURTHER PERSPECTIVES

INTRODUCTION TO KM3NeT SCIENCE

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As of June 2019: 55 institutes and groups; >250 scientists;

46 cities;17 countries; 4 continents

Prof. Dr. Harold Yepes Ramírez, NNN2019, MEDELLÍN-COLOMBIA

5Prof. Dr. Harold Yepes Ramírez, NNN2019, MEDELLÍN-COLOMBIA

MOTIVATIONEnhance our knowledge spanning Earth, Sea and Space Sciences (astro-particle physics),

taking advantage of operational experience of “Neutrino Telescopes”

OBJECTIVE (EARTH AND SEA SCIENCES):

Mediterranean deep-sea as of prime interest for marinebio- and geo-science investigations: permanent, real-timeand high-bandwidth connection to shore.

OBJECTIVES (ASTRO-PARTICLE PHYSICS):

IceCube signal (TXS Blazar), discovery and study of other HE neutrino sources in the Universe. Neutrinos Mass Hierarchy (NMH), tau-neutrino appearance.


ν-astronomy(+astrophysics)

νatm oscillation experiments PHYSICS

DETECTOR REQUIREMENTShigher densities larger volumes

NEUTRINO ENERGIES

~ MeV – 100 GeVNMH with atmospheric flux

100 GeV - 30 TeVSeveral galactic (gamma) sources

30 TeV – 3 PeVIceCube signal (astrophysical flux)

Other fluxes and energies?

ARCA (KM3NeT-It)(Astroparticle Research with Cosmics in the Abyss)

100 km off-shore Capo Passero, Depth ~ 3.4 km 40 km off-shore Toulon, Depth ~ 2.5 km

ORCA (KM3NeT-Fr)(Oscillation Research with Cosmics in the Abyss)


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Low Energy (1 < Eν [GeV] < 100)NMH, oscillation parameters, tau appearance,

sterile-ν, Non-Standard interactionsν-tomography (oscillation)

Medium Energy [10 GeV < Eν < 1 TeV]Dark Matter, exotics (monopoles, nuclearites)

High Energy (Eν [TeV] > 1)ν-astronomy/astrophysics (GRB/AGN/Blazars), MM

studies (p/ν/GW/γ), Particle physics (μatm/νatm/ντ),ν-tomography (absorption)

SuperNovae-ν (~MeV)

THE KM3NeT NEUTRINO DETECTOR


ORCA (Denser Detector)High density, low threshold optimization,

sensitivity to changes of flavour[atmospheric neutrinos]

ARCA (Sparser Detector) Large volume, low fluxes optimization,

large effective area[astrophysical neutrinos]

same technology and layout (dimensions scaled)

2 Building Blocks (BBs)[2 x 115 Detection Units (DUs)]

(~ 1 Gton instrumented)

1 Building Block (BB)[1 x 115 Detection Units (DUs)]

(~ 6 Mton instrumented)


The KM3NeT Detection Unit (DU):

18 DOM integrated on vertical slender strings tied by2 parallel Dyneema® ropes, 31x3’’ PMTs / DOM.

White Rabbit (WR) time synchronization protocol.

Backbone: 2 copper conductors; 18 fibers (+spares).

Break out of cable at each DOM.

Optical fiber transmission (Gbit/s) by base modulewith DWDM at string anchor.

All-data-to-shore concept: Filtering/Trigger on-shore in computer farm.

+ Nodes for long-term high-bandwidth connection for Earth and Sea Sciences

The KM3NeT BB:(ARCA-ORCA)

115 DUs

3D network of ~64k PMTs

~800-200 m

~1000-212 m

~36-9 m

~90-20 m


DOM Generalities

Directional SensitivitySegmented cathode area

(31x3” PMTs)+

Improved Photon CountingLight concentrator ring, cathode

area (~3x10’’ PMT)+

Less overhead, improved readout and calibration devices

Central Logic Board (+Power Board), FPGA readout, compass

and tiltmeter inside. NanoBeacon (LED systems), piezo-sensors

PMT Specifics

Timing ≤2ns (RMS)

QE≥25-30%

Collection efficiency ≥ 90%

Photon counting purity100%

Price/cm2

≤10” PMT


PHASE-I: (on-going)

Fully funded. 30 DU’s: 24 ARCA + 6 ORCA (~0.3BB). Proof of feasibility and first science results.

PHASE-II: (letter of intent)

Partially funded. 345 DU’s: 2x115 (≡2BB) ARCA + 1x115 (≡1BB) ORCA. IceCube signal, NMH, all flavour ν-physics, astronomy and

astrophysics, Dark Matter, etc.

PHASE-III: (the horizon…)

Plans … looking for funding. 690 DU’s: 6x115 (≡6BB) ARCA + P2O project + Super-ORCA in total. Extended ν-astronomy, astrophysics and particle physics program. ν-tomography.


Sea Water target material for ν interactions + Cherenkov light radiator.

ALL FLAVOUR NEUTRINO OBSERVATION: 6 orders of magnitude in E(GeV-PeV)

Reconstruction of arrival direction and energy of neutrinos:Position + timing + amplitude of the hits

Signal from νcosmic interactions (inside,outside the detection media).Background Physical (CR interactions atatmosph.) + Optical (bioluminescence + 40K).

Indirect observation Cherenkov lightinduced by outgoing charged-leptons(l) (μ, τ,

e) crossing the detector from νl-interactionswith nucleons (N) of detector surroundings.

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μ-track from CC νμ (golden channel for ν-astronomy)

TRACK-LIKE: interaction can occur far from the detectorlarge effective volume


CC tau/electron and NC all flavour(80% of all ν-interactions)

SHOWER-LIKE (bang, 2-bang?): events contained in thedetector smaller effective volume

KM3NeT PERFORMANCE


Photon counting capabilities and directional sensitivity of DOM. Eur. Phys. J. C (2014) 74:3056

Test of DU structure functionality, Test of intra-DOM and inter-DOM calibration - Eur. Phys. J. C (2016) 76:54

APRIL 2013Prototype DOM deployed at ANTARES site

May 2014Prototype DU (3 DOMs) at Capo Passero

December 2015First ARCA DU deployed in Capo Passero

Muon flux dependence on depth, DU calibration, Trigger implementation, Track reconstruction + MC comparison …

ACTUALLY?


REQUIREMENTS OF THE DETECTOR:

• Timing Relative hit times accuracy ~ 1 ns• Positioning / Orientation DOM position accuracy < 20 cm (distance traveled by

Cherenkov photons in 1 ns) / PMT orientation accuracy < 3°• Optical Effect of λabs, λsca, λtr , η accounted in the design (OCS TBD)

AN OUTSTANDING DESIGN, A PROPERLY CALIBRATED DETECTOR …

ARCA GOALS: High-energy neutrino sources (Eν > 10 TeV)

• Track-like events (muons) α (median) < 0.2°, ΔE ~ 0.3• Shower-like events α (median) < 2°, ΔE ~ 0.1

ORCA GOALS: NMH and oscillation parameters (MeV < Eν < GeV)

• Angular resolution and effective area depending on the energy threshold.


Nanosecond synchronization (WR protocol) of Δt of Cherenkov light signals recorded byPMTs: intra-DOM, inter-DOM, inter-DU.

Effect of timing uncertainties (MC)in addition to standard PMT TTS

(E-2 spectrum with E > 10 TeV)

Requirements On-shore calibration (Dark Room) In-situ calibration

DU integration, testing and calibration↓

Equalization of PMT gain ~ 3x106 at 0.3 spe(start time + ToT PMT data)

↓

Inter/Intra-DOM calibration(blue laser flashes simultaneously 1-2 PMTs/DOM)

Intra-DOM calibration(40K method)

↓

Inter-DOM calibration(NanoBeacon)

(Down-going muons)↓

Inter-DU calibration(Down-going muons)

Time offset difference between the 2 reference PMTs for each DOM


Positions of DOMs are recovered through a RelativeAcoustic Positioning System:

1. A Long Base Line element of acoustic Tx (beacons) andRx (Digital Acoustic Receivers) at known positions.

2. An array of piezo-electric Digital Acoustic Receiversinstalled along the DUs (into each DOM).

3. A farm of computers for the analysis of acoustic data.

Orientation through compass installed in each DOM.

The DU shape and the DOM position is known at the level

of few cm!

PMT orientation accuracy also reached …

KM3NeT preliminary

KM3NeT preliminary

KM3NeT FIRST DATA AND FURTHER PERSPECTIVES


DATA SAMPLE:

ORCA1: 09/11/2017 – 13/12/2017(+2019)ARCA2: 23/12/2016 – 03/02/2017

Parametrization of the underwater muon flux by Bugaev et al.

Energy losses in seawater↓

Lower rate of atmospheric muons↓

Effect on coincidence rates

Muon flux attenuation over more than 1 km length

RMS < 2%Proved calibration and PMT detection efficiency

Coincidence rate ∝muon flux × normalization factor

ORCA

ARCA


time

ARCA:6 up-going neutrino candidates

[cos(zenith_reco)<-0.8]

ORCA:11 up-going neutrino candidates

[cos(zenith_reco)<-0.8]

KM3NeT is able to perform an outstanding reconstruction with only a few lines and short lifetime !!!

R. Coniglione. PoS, Volume 358, 36th International Cosmic Ray Conference 2019


Credits to Rodrigo G. Ruiz, NIKHEF, KM3NeT at Lake Louise Winter Institute 2019


Discovery at 5σ significance in less than one year !!!

Excellent sensitivity (E-2) at southern hemisphere

P. Sapienza, A. Trovato. Astroparticle Physics 111 (2019) 100

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Atmospheric ν-flux


Known composition of νμ , νe

ν-propagation through Earth ν-oscillation pattern

Wide range of SBL-LBL (50-12742 km) and Eν (GeV PeV)

Distortion by Earth matter effects(NMH-dependence): max. diff. NH↔ IH for resonance in Earth mantle θ = 130° (7645 km), Eν = 7 GeV

Akhmedov, Razzaque & Smirnov, JHEP 02 (2013) 082

Measure zenith angle and energy of up-going νatm (~GeV)

(identify and count νμ and νe channel events)


Sensitivity to distinguish between NH↔ IH: ~3σ in 3 years (median sensitivity)

IH, 1 contours

Competitive measurements of Δm232 (2-3%

precision) and sin2θ23 (4-10% precision)

R. Coniglione. PoS, Volume 358, 36th International Cosmic Ray Conference 2019


Baseline at L = 2595 km (νe appearance)Beam inclination horizontal/vertical = 21.7°/11.8˚ (cos θ = 0.2)

Deepest point 134 km = 3.3 g/cm3First oscillation maximum = 5.1 GeV

Target energy range = 3-8 GeV

U70 (constructed in 1967)1.5 km circumference

Current operation at 8 - 15 kW1-turn fast extraction: 5 μs spill every 9 s


D. Zaborov et al., Eur. Phys. J. C (2019) 79:758

3 yrs. at 90 kW to reach ≥ 3σ sensitivity, for any value of θ23 [40°, 50°] and any value of δCP

Phase 1: NMHORCA detector + 1(5) years of running

at 450(90) kW beam power

Phase 2: δCP

10x denser detector (Super ORCA) running at 450 kW; δCP to 10-16° in 10 yrs

Best precision for δCP = 0°, 180° with resolution σδ ≈ 10° (10 yrs) and δCP =

90°, 270° with σδ ≈ 16°


TECHNICAL ASPECTS:

1. Operational experience, technical and scientific outcomes of previous MediterraneanNeutrino Telescopes have been fundamental for KM3NeT.

2. Mass production phase has started, integration and deployment of DUs will be pursued ata continuous pace, at the highest priority level.

KM3NeT SCIENCE PROGRAMS:

1. Discovery of astrophysical neutrino sources at 5σ significance in less than one year.Excellent sensitivity at southern hemisphere and field of view to Galactic sources.

2. Sensitivity to NMH ~3σ in 3 years. Competitive measurements of Δm232 and sin2θ23.

KM3NeT EXTERNAL SIDE-PROJECTS:

P2O will allow (~ 3 yrs. at 90 kW) to reach ≥ 3σ sensitivity, for any value of θ23 and δCP.

Prof. Dr. Harold Yepes Ramírez ([email protected])KM3NeT-EC Principal Investigator (http://www.km3net.org/)

LASF4RI National Representative (https://lasf4ri.org/)

http://www.km3net.org/

https://lasf4ri.org/

introduction to km3net science · prof. dr. harold yepes ramírez, nnn2019, medellÍn-colombia...

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